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High Energy cosmic-Radiation Detection (HERD) Facility onboard
China’s Space Station
Shuang-Nan Zhang ( 张双南 )[email protected]
Center for Particle Astrophysics粒子天体物理中心
Institute of High Energy PhysicsChinese Academy of Sciences
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Astroparticle Physics & Particle Astrophysics
Physics
Particle Physics
Particle Astrophysics Astroparticle Physics
Astronomy
Astrophysics
Tool: Universe
Goal: Particle Physics
Tool: Particle Physics
Goal: Universe
The Physical Universe and Its Laws
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IHEP Center for Particle
Astrophysics
High Energy Cosmic-rayCharged Particles,
Neutrinos, Gamma-raysExplosive Phenomena
GRB,SN&SNRBH&NS accretion
Sea Level and Underground Exp.CMS, Daya-Bay
Dark Matter Search
Gravity & CosmologyCompact ObjectsGalaxy, Cluster
CMB
Space ProjectsAMS, CE, HXMT
POLAR, DAMPE, SVOMSEMS, XTP, HERD
Tibet High Altitude Cosmic-ray Observatory
YBJ － AS, ARGOLHAASO
180 fulltime staff scientists and engineers
150 students, postdocs and visiting scholars
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Science goals Mission requirements
Dark matter search
R1: Better statistical measurements of e/γ between 100 GeV to 10 TeV
Origin of Galactic Cosmic rays
R2: Better spectral and composition measurements of CRs between 300 GeV to PeV* with a large geometrical factor
HERD: High Energy cosmic-Radiation Detector
Secondary science: γ-ray astronomy monitoring of GRBs, microquasars, Blazars and other transients down to 100 MeV for γ -rays plastic scintillator shields for γ -ray selection*complementary to high altitude cosmic-ray observations
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HERD Cosmic Ray Capability Requirement
P (<A> ~ 1)He (<A> ~ 4)L (<A> ~ 8)M (<A> ~ 14)H (<A> ~ 25)VH (<A> ~ 35) Fe (<A> ~ 56)
Except for L, up to PeV spectra feasible with
GF~2-3 in ~years: discriminate between models.
N(E
>E
0; 2
yr) PeV
PeV
Model 1Light model
Model 2Heavy Model
TeV TeV
PeV PeV
HERD HERD
Detection limit: N = 10 events
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Characteristics of all components
type size X0,λ unit main functionstracker(top)
Si strips
70 cm ×70 cm
2 X0 7 x-y(W foils)
ChargeEarly showerTracks
tracker4 sides
Si strips
65 cm ×50 cm
2 X0 7 x-y(W foils)
ChargeEarly showerTracks
CALO ~10KLYSO cubes
63 cm ×63 cm ×63 cm
55 X03 λ
3 cm ×3 cm ×3 cm
e/γ energynucleon energye/p separation
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Expected performance of HERD
γ/e energy range (CALO) tens of GeV-10TeV
nucleon energy range (CALO) up to PeV
γ/e angular resol. 0.1o
nucleon charge resol. 0.1-0.15 c.u
γ/e energy resolution (CALO) <1%@200GeVproton energy resolution (CALO) 20%
e/p separation power (CALO) <10-5
electron eff. geometrical factor (CALO) 3.7 m2sr@600 GeV
proton eff. geometrical factor (CALO) 2.6 m2sr@400 TeV
Acceptance & H-energy > n10X all others
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Other detectors: Top down “small” FoV
ISS-CREAM: 2017?
ISS-CALET: 2015
ISS-AMS: 2011
DAMPE2015
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HERD Design ： 3D Calo & 5-Side Sensitive
n10X acceptance than others, but weight 2.3 T ~1/3 AMS
3D CALOe/G/CR energye/p discriminationSTK(W+SSD)
STK(W+SSD)Chargegamma-ray directionCR back scatter
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Simulation results: energy resolutions
Electron < 1%; Proton: ~20%Essential for spectral features!
Electrons
Protons
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Energy Resolution for gamma-rays
500 MeV-100 GeV result
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HERD Eff. Geometrical Factor: CALO
All five sidesAll five sides
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PAMELA: 2006-2016 CALET: 2015-2020; AMS: 2011-2021; DAMPE: 2015-2020; Fermi: 2008-2018; HERD: 2020-2021
HERD sensitivity to gamma-ray line
HERD 1 yr
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000
00
Z
DM annihilation line of HERD
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Expected HERD Proton and He Spectra
Horandel model as HERD inputOnly statistical error
Protons
He
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Expected HERD Spectra of C and Fe
C
Fe
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Gamma-ray Sky Survey Sensitivity
Narrow FoV
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CALO readout
Trigger
Fast FrameCCD
Optical Coupling
Image Intensifier
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Proof of principle
2×2×6 CsI crystal array
ICCD image of cosmic ray events
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HERD progress – ICCD development
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Scintillator signal readouts• LYSO scintillator WLSF
• Fiber to ICCD system
Image intensifier
Taper
ICCD system
Optical fiber winding Crystal packing
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Fiber Image on CCD
Signal: 3000 pe; gain of image intensifier: 4000
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Fiber Image on CCD
Signal: 3000 pe; gain of image intensifier: 50000
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CERN Beam Test in Nov 10-20, 2015
• SPS H4: P & Pb
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Design of the prototype
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Requirements on the prototype
• Requirement on dynamic range: ~6000– Starting from 1/3 MIPs=10 MeV– Ending at max. energy deposition: 60 GeV
• Requirement on frame rate of ICCD: > 500 fps– Since the electrons arrive randomly in time
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Requirements on the prototype• Scale of the prototype ： 5×5×10, 3×3×3 cm3
– Larger than envelope of 280 GeV e- shower– 36% of the total energy for protons
1/40 size of HERD
Along the beam
Transverse direction27/42
LYSO light output
for 3cm×3cm×3cm cubic LYSO, but signal << 30 MeV MIP
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LYSO performance
Variation of LYSO light output:(Max-Min)/Mean ≈25%
Energy resolution (σ/E) for 662keV γ peak:< 5%
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Realization of two readout ranges
T HLow
Low H
T
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Signal ratios ~ 50:1
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Fiber winding development
Slot instead of holeFiber insert hole
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Fiber winding development
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Fiber winding development
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Fiber winding development
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Fiber winding development
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Making ESR wrapping
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Assembly and lab test of the prototype
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1st HERD workshop, Oct.17-18, 2012, IHEP, Beijing
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2nd HERD Workshop @IHEP 2013/12/2-3
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Beam test preparation meeting 2015/08/31@Rome
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The HERD Proto-Collaboration Team• Chinese institutions (more welcome!)
– Institute of High Energy Physics, Purple Mountain Observatory, Xi’an Institute of Optical and Precision Mechanics, University of Science and Technology of China, Nanjing University, Peking University, Yunnan University, China University of Geosciences, Ningbo University, Guangxi University
• International institutions (more welcome!)– Switzerland: University of Geneva– Italy: Università di Pisa/INFN, IAPS/INAF, University of
Florence/INFN, University of Perugia/INFN, University of Trento/INFN, University of Bari/INFN, University of Salento/INFN-Lecce
– Sweden: KTH– USA: MIT/Harvard
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SPIE, 9144, id. 91440X 9 pp. (2014)
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